基于SHARK星系模拟的LISA和PTA预测
Predictions for LISA and PTA based on SHARK galaxy simulations
摘要：
我们提出了我们的分析的一组人口的大规模黑洞（MBH）的二进制文件中产生的星系演化的半解析模型（SHARK）。我们专注于研究MBH合并过程中产生的引力波（GW）发射，在他们的探测能力与当前和未来的探测器，即脉冲星定时阵列（PTA）和激光干涉仪空间天线（LISA）。SHARK的主要优点是，它提供了一种在一致的框架内探索MBH和星系演化过程的一些不同模型的方法，并且还成功地对电磁观测的当前限制进行了测试。在我们的工作中，我们研究了12个不同的模型，在他们的MBH种子形成的情况下，我们测试了两个不同的MBH增长和反馈模型。根据我们的估计，我们发现，LISA将能够检测到几个到几十个合并事件，每年的最大和最小规模的种子场景，分别。我们还表明，这种关系的强度取决于MBH增长模型，在最极端的情况下，我们发现两倍的检测到的事件相同的初始种子质量。最后，我们估计在nHz频率的GW背景的振幅为$1.4\cdot10^{-16} - 1.1\cdot10^{-15}$的顺序。这个值完全取决于星系合并和它们的MBH之间的时间延迟。
英文摘要：
We present our analysis of a set of populations of massive black hole (MBH) binaries generated in the recent semi-analytic model of galaxy evolution (SHARK). We focus on studying gravitational wave (GW) emission produced during MBH mergers in terms of their detectability with current and future detectors, namely, Pulsar Timing Arrays (PTAs) and Laser Interferometer Space Antenna (LISA). The key advantage of SHARK is that it provides a way to explore a number of distinct models of MBH and galaxy evolution processes within a consistent framework and it was also successfully tested against current constraints from electromagnetic observations. In our work, we studied 12 models that vary in terms of their MBH seed formation scenarios and we tested two different MBH growth and feedback models. Based on our estimates, we find that LISA will be able to detect several to several tens of merger events per year for the most and least massive seed scenarios, respectively. We also show that the strength of this relation depends on the MBH growth model, where in the most extreme case, we find twice as many detected events for the same initial seed masses. Finally, we estimated the amplitude of the GW background at nHz frequencies to be on the order of $1.4\cdot10^{-16} - 1.1\cdot10^{-15}$. This value depends solely on the time delay between the merger of galaxies and their MBHs.
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